We present results from our Giant Metrewave Radio Telescope (GMRT) Hi, Himalayan Chandra Telescope (HCT) Hα, 1 m Sampurnanand Telescope (ST) and 1.3 m Devasthal Fast Optical Telescope (DFOT) deep optical observations of the NGC 7805/6 (Arp 112) system to test KUG 2359+311’s tidal dwarf galaxy (TDG) candidacy and explore the properties of the interacting system. Our GMRT H I map shows no H I detection associated with KUG 2359+311, nor any H I tail or bridge-like structure connecting KUG 2359+311 to the NGC 7805/6 system. Our HCT Hα image, on the other hand, displays strong detections in KUG 2359+311, with net SFR ∼ 0.035 0.009 M _⊙ yr⁻¹. The Hα data constrain the redshift of KUG 2359+311 to 0.00 ≤ z ≤ 0.043, compared to the redshift of NGC 7806 of ∼ 0.015. TDGs detected to date have all been H i rich, and displayed H i, ionised gas and stellar tidal debris trails (bridges or tails) linking them to their parent systems. However, neither our H i data nor our optical imaging, while three magnitudes deeper than SDSS, reveals a tidal trail connecting KUG 2359+311 to NGC 7805/6. Lack of H i, presence of an old stellar population, ongoing star formation and reasonably high SFR compared to normal dwarf galaxies suggest that KUG 2359+311 may not be an Arp 112 TDG. It is most likely a case of a regular gas-rich dwarf galaxy undergoing a morphological transformation after having lost its entire gas content to an interaction with the Arp 112 system. Redshift and metallicity from future spectroscopic observations of KUG 2359+311 would help clarify the nature of this enigmatic structure.

我们展示了我们的巨型米波射电望远镜 (GMRT) H i、喜马拉雅钱德拉望远镜 (HCT) H α、1 m Sampurnanand 望远镜 (ST) 和 1.3 m Devasthal 快速光学望远镜 (DFOT) 对 NGC 7805/6 的深度光学观测的结果(Arp 112) 系统测试 KUG 2359+311 的潮汐矮星系 (TDG) 候选资格并探索相互作用系统的特性。我们的 GMRT HI 地图没有显示与 KUG 2359+311 相关的 HI 检测，也没有任何 HI 尾或将 KUG 2359+311 连接到 NGC 7805/6 系统的类似桥的结构。另一方面，我们的 HCT H α图像在 KUG 2359+311中显示出强检测，净 SFR ∼ 0.035 0.009 M⊙ _yr ^-1。Hα _数据将 KUG 2359+311 的红移限制在 0.00 ≤ z ≤ 0.043，而 NGC 7806 的红移约为 0.015。迄今为止检测到的 TDG 都富含H i ，并显示出 H i、电离气体和恒星潮汐碎片轨迹（桥或尾），它们将它们与母系统联系起来。然而，无论是我们的 H i数据还是我们的光学成像，虽然都比 SDSS 深三个数量级，但都没有揭示连接 KUG 2359+311 和 NGC 7805/6 的潮汐轨迹。缺乏HI，与正常矮星系相比，存在一个古老的恒星群、持续的恒星形成和相当高的恒星形成率表明，KUG 2359+311 可能不是 Arp 112 TDG。这很可能是一个规则的富含气体的矮星系在与 Arp 112 系统的相互作用失去其全部气体含量后经历形态转变的情况。未来对 KUG 2359+311 的光谱观测的红移和金属丰度将有助于阐明这种神秘结构的性质。